Abstract
AbstractThis contribution provides a review of our current understanding of radio source populations and their host galaxies, as derived from studies of the local Universe, in particular using the Sloan Digital Sky Survey. Evidence is presented that low luminosity radio sources are fundamentally distinct objects to high radio luminosity sources and optically or X‐ray selected AGN, suggesting that these are fuelled by a different mechanism. The low‐luminosity radio sources are argued to be fuelled by the accretion of hot gas from their surrounding X‐ray haloes, and this offers a potential feedback loop via which the radio‐loud AGN can control the cooling of the hot gas, and thus the growth of their host galaxy. The energetic output of the radio sources is derived in order to show that this is indeed feasible. It is emphasised that the difference between these two modes of AGN fuelling is distinct from that of the two different radio morphological classes of radioloud AGN (Fanaroff‐Riley classes 1 and 2). The origin of the FR‐dichotomy is investigated using Sloan data, and argued to be associated with the environment and evolution of the radio sources. Finally, the role of CSS and GPS sources within this picture is discussed (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
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